A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction

Autores
Maeda, Keiichi; Chandra, Poonam; Moriya, Takashi J.; Reguitti, Andrea; Matsuoka, Tomoki; Michiyama, Tomonari; Pignata, Giuliano; Hiramatsu, Daichi; Azalee Bostroem, K.; Kundu, Esha; Kuncarayakti, Hanindyo; Bersten, Melina Cecilia; Pooley, David; Lee, Shiu Hang; Patnaude, Daniel; Rodríguez, Ósmar; Folatelli, Gaston
Año de publicación
2022
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
SN 2018ivc is an unusual Type II supernova (SN II). It is a variant of SNe IIL, which might represent a transitional case between SNe IIP with a massive H-rich envelope and SNe IIb with only a small amount of the H-rich envelope. However, SN 2018ivc shows an optical light-curve evolution more complicated than that of canonical SNe IIL. In this paper, we present the results of prompt follow-up observations of SN 2018ivc with the Atacama Large Millimeter/submillimeter Array. Its synchrotron emission is similar to that of SN IIb 1993J, suggesting that it is intrinsically an SN IIb-like explosion of an He star with a modest (∼0.5-1M ⊙) extended H-rich envelope. Its radio, optical, and X-ray light curves are explained primarily by the interaction between the SN ejecta and the circumstellar material (CSM); we thus suggest that it is a rare example (and the first involving the “canonical” SN IIb ejecta) for which the multiwavelength emission is powered mainly by the SN-CSM interaction. The inner CSM density, reflecting the progenitor activity in the final decade, is comparable to that of SN IIb 2013cu, which shows a flash spectral feature. The outer CSM density, and therefore the mass-loss rate in the final ∼200 yr, is higher than that of SN 1993J by a factor of ∼5. We suggest that SN 2018ivc represents a missing link between SNe IIP and SNe IIb/Ib/Ic in the binary evolution scenario.
Fil: Maeda, Keiichi. Kyoto University; Japón
Fil: Chandra, Poonam. National Radio Astronomy Observatory; Estados Unidos
Fil: Moriya, Takashi J.. Monash University; Australia
Fil: Reguitti, Andrea. Universidad Andrés Bello; Chile
Fil: Matsuoka, Tomoki. Kyoto University; Japón
Fil: Michiyama, Tomonari. Osaka University; China
Fil: Pignata, Giuliano. Universidad Andrés Bello; Chile
Fil: Hiramatsu, Daichi. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Azalee Bostroem, K.. The George Washington University; Estados Unidos
Fil: Kundu, Esha. Michigan State University; Estados Unidos
Fil: Kuncarayakti, Hanindyo. Turun Yliopisto; Finlandia
Fil: Bersten, Melina Cecilia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Pooley, David. Trinity College; Estados Unidos
Fil: Lee, Shiu Hang. Kyoto University; Japón
Fil: Patnaude, Daniel. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Rodríguez, Ósmar. Universitat Tel Aviv; Israel
Fil: Folatelli, Gaston. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Materia
SUPERNOVAE
CIRCUMSTELLAR MATTER
Radio Sources
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/210934
Acceder
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network_name_str CONICET Digital (CONICET)
spelling A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar InteractionMaeda, KeiichiChandra, PoonamMoriya, Takashi J.Reguitti, AndreaMatsuoka, TomokiMichiyama, TomonariPignata, GiulianoHiramatsu, DaichiAzalee Bostroem, K.Kundu, EshaKuncarayakti, HanindyoBersten, Melina CeciliaPooley, DavidLee, Shiu HangPatnaude, DanielRodríguez, ÓsmarFolatelli, GastonSUPERNOVAECIRCUMSTELLAR MATTERRadio Sourceshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1SN 2018ivc is an unusual Type II supernova (SN II). It is a variant of SNe IIL, which might represent a transitional case between SNe IIP with a massive H-rich envelope and SNe IIb with only a small amount of the H-rich envelope. However, SN 2018ivc shows an optical light-curve evolution more complicated than that of canonical SNe IIL. In this paper, we present the results of prompt follow-up observations of SN 2018ivc with the Atacama Large Millimeter/submillimeter Array. Its synchrotron emission is similar to that of SN IIb 1993J, suggesting that it is intrinsically an SN IIb-like explosion of an He star with a modest (∼0.5-1M ⊙) extended H-rich envelope. Its radio, optical, and X-ray light curves are explained primarily by the interaction between the SN ejecta and the circumstellar material (CSM); we thus suggest that it is a rare example (and the first involving the “canonical” SN IIb ejecta) for which the multiwavelength emission is powered mainly by the SN-CSM interaction. The inner CSM density, reflecting the progenitor activity in the final decade, is comparable to that of SN IIb 2013cu, which shows a flash spectral feature. The outer CSM density, and therefore the mass-loss rate in the final ∼200 yr, is higher than that of SN 1993J by a factor of ∼5. We suggest that SN 2018ivc represents a missing link between SNe IIP and SNe IIb/Ib/Ic in the binary evolution scenario.Fil: Maeda, Keiichi. Kyoto University; JapónFil: Chandra, Poonam. National Radio Astronomy Observatory; Estados UnidosFil: Moriya, Takashi J.. Monash University; AustraliaFil: Reguitti, Andrea. Universidad Andrés Bello; ChileFil: Matsuoka, Tomoki. Kyoto University; JapónFil: Michiyama, Tomonari. Osaka University; ChinaFil: Pignata, Giuliano. Universidad Andrés Bello; ChileFil: Hiramatsu, Daichi. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Azalee Bostroem, K.. The George Washington University; Estados UnidosFil: Kundu, Esha. Michigan State University; Estados UnidosFil: Kuncarayakti, Hanindyo. Turun Yliopisto; FinlandiaFil: Bersten, Melina Cecilia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Pooley, David. Trinity College; Estados UnidosFil: Lee, Shiu Hang. Kyoto University; JapónFil: Patnaude, Daniel. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Rodríguez, Ósmar. Universitat Tel Aviv; IsraelFil: Folatelli, Gaston. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaIOP Publishing2022-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/210934Maeda, Keiichi; Chandra, Poonam; Moriya, Takashi J.; Reguitti, Andrea; Matsuoka, Tomoki; et al.; A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction; IOP Publishing; Astrophysical Journal; 942; 1; 12-2022; 1-310004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/aca1b7info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aca1b7info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:35:26Zoai:ri.conicet.gov.ar:11336/210934instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 09:35:26.313CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction
title A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction
spellingShingle A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction
Maeda, Keiichi
SUPERNOVAE
CIRCUMSTELLAR MATTER
Radio Sources
title_short A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction
title_full A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction
title_fullStr A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction
title_full_unstemmed A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction
title_sort A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction
dc.creator.none.fl_str_mv Maeda, Keiichi
Chandra, Poonam
Moriya, Takashi J.
Reguitti, Andrea
Matsuoka, Tomoki
Michiyama, Tomonari
Pignata, Giuliano
Hiramatsu, Daichi
Azalee Bostroem, K.
Kundu, Esha
Kuncarayakti, Hanindyo
Bersten, Melina Cecilia
Pooley, David
Lee, Shiu Hang
Patnaude, Daniel
Rodríguez, Ósmar
Folatelli, Gaston
author Maeda, Keiichi
author_facet Maeda, Keiichi
Chandra, Poonam
Moriya, Takashi J.
Reguitti, Andrea
Matsuoka, Tomoki
Michiyama, Tomonari
Pignata, Giuliano
Hiramatsu, Daichi
Azalee Bostroem, K.
Kundu, Esha
Kuncarayakti, Hanindyo
Bersten, Melina Cecilia
Pooley, David
Lee, Shiu Hang
Patnaude, Daniel
Rodríguez, Ósmar
Folatelli, Gaston
author_role author
author2 Chandra, Poonam
Moriya, Takashi J.
Reguitti, Andrea
Matsuoka, Tomoki
Michiyama, Tomonari
Pignata, Giuliano
Hiramatsu, Daichi
Azalee Bostroem, K.
Kundu, Esha
Kuncarayakti, Hanindyo
Bersten, Melina Cecilia
Pooley, David
Lee, Shiu Hang
Patnaude, Daniel
Rodríguez, Ósmar
Folatelli, Gaston
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv SUPERNOVAE
CIRCUMSTELLAR MATTER
Radio Sources
topic SUPERNOVAE
CIRCUMSTELLAR MATTER
Radio Sources
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv SN 2018ivc is an unusual Type II supernova (SN II). It is a variant of SNe IIL, which might represent a transitional case between SNe IIP with a massive H-rich envelope and SNe IIb with only a small amount of the H-rich envelope. However, SN 2018ivc shows an optical light-curve evolution more complicated than that of canonical SNe IIL. In this paper, we present the results of prompt follow-up observations of SN 2018ivc with the Atacama Large Millimeter/submillimeter Array. Its synchrotron emission is similar to that of SN IIb 1993J, suggesting that it is intrinsically an SN IIb-like explosion of an He star with a modest (∼0.5-1M ⊙) extended H-rich envelope. Its radio, optical, and X-ray light curves are explained primarily by the interaction between the SN ejecta and the circumstellar material (CSM); we thus suggest that it is a rare example (and the first involving the “canonical” SN IIb ejecta) for which the multiwavelength emission is powered mainly by the SN-CSM interaction. The inner CSM density, reflecting the progenitor activity in the final decade, is comparable to that of SN IIb 2013cu, which shows a flash spectral feature. The outer CSM density, and therefore the mass-loss rate in the final ∼200 yr, is higher than that of SN 1993J by a factor of ∼5. We suggest that SN 2018ivc represents a missing link between SNe IIP and SNe IIb/Ib/Ic in the binary evolution scenario.
Fil: Maeda, Keiichi. Kyoto University; Japón
Fil: Chandra, Poonam. National Radio Astronomy Observatory; Estados Unidos
Fil: Moriya, Takashi J.. Monash University; Australia
Fil: Reguitti, Andrea. Universidad Andrés Bello; Chile
Fil: Matsuoka, Tomoki. Kyoto University; Japón
Fil: Michiyama, Tomonari. Osaka University; China
Fil: Pignata, Giuliano. Universidad Andrés Bello; Chile
Fil: Hiramatsu, Daichi. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Azalee Bostroem, K.. The George Washington University; Estados Unidos
Fil: Kundu, Esha. Michigan State University; Estados Unidos
Fil: Kuncarayakti, Hanindyo. Turun Yliopisto; Finlandia
Fil: Bersten, Melina Cecilia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Pooley, David. Trinity College; Estados Unidos
Fil: Lee, Shiu Hang. Kyoto University; Japón
Fil: Patnaude, Daniel. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Rodríguez, Ósmar. Universitat Tel Aviv; Israel
Fil: Folatelli, Gaston. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
description SN 2018ivc is an unusual Type II supernova (SN II). It is a variant of SNe IIL, which might represent a transitional case between SNe IIP with a massive H-rich envelope and SNe IIb with only a small amount of the H-rich envelope. However, SN 2018ivc shows an optical light-curve evolution more complicated than that of canonical SNe IIL. In this paper, we present the results of prompt follow-up observations of SN 2018ivc with the Atacama Large Millimeter/submillimeter Array. Its synchrotron emission is similar to that of SN IIb 1993J, suggesting that it is intrinsically an SN IIb-like explosion of an He star with a modest (∼0.5-1M ⊙) extended H-rich envelope. Its radio, optical, and X-ray light curves are explained primarily by the interaction between the SN ejecta and the circumstellar material (CSM); we thus suggest that it is a rare example (and the first involving the “canonical” SN IIb ejecta) for which the multiwavelength emission is powered mainly by the SN-CSM interaction. The inner CSM density, reflecting the progenitor activity in the final decade, is comparable to that of SN IIb 2013cu, which shows a flash spectral feature. The outer CSM density, and therefore the mass-loss rate in the final ∼200 yr, is higher than that of SN 1993J by a factor of ∼5. We suggest that SN 2018ivc represents a missing link between SNe IIP and SNe IIb/Ib/Ic in the binary evolution scenario.
publishDate 2022
dc.date.none.fl_str_mv 2022-12
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/210934
Maeda, Keiichi; Chandra, Poonam; Moriya, Takashi J.; Reguitti, Andrea; Matsuoka, Tomoki; et al.; A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction; IOP Publishing; Astrophysical Journal; 942; 1; 12-2022; 1-31
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/210934
identifier_str_mv Maeda, Keiichi; Chandra, Poonam; Moriya, Takashi J.; Reguitti, Andrea; Matsuoka, Tomoki; et al.; A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction; IOP Publishing; Astrophysical Journal; 942; 1; 12-2022; 1-31
0004-637X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/aca1b7
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aca1b7
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.070432

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